Xing Zh., Zhou Sh. Neutrinos in Particle Physics, Astronomy and Cosmology

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Zhi-Zhong

Shun Zhou

Neutrinos in Particle Physics,

Astronomy and Cosmology

With 61 ﬁgures

Authors

Prof. Dr. Zhi-Zhong Xing Dr. Shun Zho

Institute o

h Ener

y Physics, Institute o

h Ener

y Physics,

Chinese

cadem

of Sciences, Chinese

cadem

of Sciences

Beijing 100049, China Beijing 100049, China

-mail: xin

ihep.ac.cn E-mail: zhoush

ihep.ac.cn

ax-Planck-Institut f¨ur Physi

(

Werner-Heisenberg-Institut

-80805 M¨unchen, German

E-mail: zhoush@mppmu.mpg.d

ISSN 1995-6819 e-ISSN 1995-6827

dvanced Topics in Science and Technology in China

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er Heidelber

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eutrinos are a kind of electrically neutral and extremely light spin-1

2 parti-

es w

ave wea

gravitationa

interactions wit

matter. T

eir

istinctive properties make them become one o

Nature’s most m

steriou

essen

ers. Since the birth of neutrino physics in 1930, when Wolf

Pauli

postulated the existence of neutrinos as a “desperate remedy” for the con

tinuous ener

y spectrum o

serve

in t

eta

ecay, intri

uin

puzz

es an

exciting discoveries have been associated with elusive neutrinos in nuclea

ysics, partic

ysics, astronomy an

cosmo

ogy.

Enrico Fermi took advanta

Pauli’s neutrino hypothesis and invented

n eﬀective theor

of weak interactions in 1933. There were several milestone

ssociated with neutrinos in the subsequent development of particle physics

The discover

electron antineutrinos

rom nuclear reactors was made b

Clyde Cowan and Frederick Reines in 1956. In the same year Tsung-Dao Le

hen Nin

Yan

published a seminal paper on parity violation in wea

nteractions, which was soon con

ﬁ

rmed by a number o

ele

ant experiments

Motivated by the experimental fact that neutrinos were almost massless an

t-handed, Richard Fe

nman and Murra

ell-Mann proposed th

−

theor

of weak interactions in 1958. Leon Lederman, Melvin Schwartz and

ack Steinberger discovered the muon neutrino, a sister of the electron neu

trino, by doin

the

ﬁ

rst hi

h-ener

y accelerator neutrino experiment in 1962.

uniﬁed

e theory of electroma

netic and weak interactions, the so-calle

tandard model

(

)

, was established by Sheldon Glashow, Steven Weinber

bdus Salam in the 1960’s. This theor

was experimentall

veriﬁed i

973, thanks to the discover

of neutral-current interactions via the neutrino-

electron and antineutrino-electron scattering. The massive mediators of weak

nteractions

(

i.e.

bosons

)

were ﬁnally observed by Carlo Rubbi

nd Simon van der Meer in 1983

n this book we start with the SM and elaborate on the intrinsic prop-

es a

dfu

lin

act

sof

ass

ess

eut

rin

.Th

s to seve

ompelling neutrino oscillation experiments done in the 1990’s and 2000’s, we

IPre

re now convinced that neutrinos are massive and lepton

ﬂ

avors are mixed

Generally speakin

, one has to rely on a speciﬁc neutrino mass model whe

iscussing massive neutrinos an

eir interactions wit

matter. But our mai

trate

yisto

ocus on the model-independent properties o

elusive neutrinos,

uch as their electromagnetic dipole moments, ﬂavor mixing, CP violatio

nd oscillations in vacuum and matter. To address the origin of ﬁnite neu-

trino masses, we s

concentrate on various seesaw mec

anisms w

ave

urrently attracted a lot of interest for model building. By choosing these

kinds of topics, we hope to keep us and the readers of our book as close as

possible to the true theor

massive neutrinos.

Furthermore, we aim to give an introduction to two newly develope

branches o

astronomy and cosmolo

y—

eutr

no astronom

neutrino

osmolo

.Thesub

ects o

neutrino astronom

include the studies o

reli

eutrinos of the Big Bang, stellar neutrinos, supernova neutrinos and high-

ener

y cosmic neutrinos.

uch studies may help us to deeply understand th

rucial role o

neutrinos in the evolution o

the Universe, the nuclear burnin

echanism of stars in their interiors, the dynamics of supernova explosions

the ori

in o

ultrahi

h-ener

ycosmicraysand

amma rays, and so on.

ar solar neutrinos have been well investi

ated. The deﬁcit of solar neutrinos,

which was ﬁrst observed by Raymond Davis in 1968, provided us with the ﬁrst

experimental evidence for the phenomenon of neutrino oscillations.

nother

ilestone in neutrino astronom

was the observation of a neutrino burst

rom the Supernova 1987A explosion in the Kamiokande-II experiment led

Masatos

iKos

a. Davis an

Kos

a receive

eNo

Prize in P

sic

n 2002 for their revolutionar

contributions to neutrino astronom

. With th

evelopment of more advanced experimental technologies, more discoveries

nd breakthroughs in neutrino astronomy are highly anticipated in the

(

near

)

uture. In particular, every eﬀort is being made to detect the cosmic neutrin

roun

, supernova neutrinos an

tra

-ener

y cosmic neutrinos

s an important branch of cosmolo

y, neutrino cosmolo

y describes th

ost profound interplay between neutrino physics and cosmology. The re

arkable success o

the standard Bi

Ban

model o

cosmolo

yhasprovedth

rucial role o

neutrinos in the primordial nucleos

nthesis, in the anisotropie

of the cosmic microwave background radiation, in the formation of the large-

e structures, an

so on. T

e cosmic neutrino

roun

neutrino

ark matter are also hot topics in cosmolo

y. In addition, the production

nd decays of heavy Majorana neutrinos in the very early Universe might be

responsible

or the ori

in o

cosmolo

ical matter-antimatter asymmetry via

the lepto

enesis mechanism. We foresee that more reliable knowled

eonthe

properties of massive neutrinos to be obtained from a variety of new experi

ts w

ill

ow us to u

sta

eof

eut

rin

eevo

of t

niverse in a better wa

and to a better level. On the other hand, the devel-

opment of neutrino cosmology is likely to provide us with more compelling

ormation about neutrino masses,

ﬂ

avor mixin

and

P violation

Pre

ace

he text o

this book can be divided into two parts: the

ﬁ

rst part consist

of chapters 1—5 and is devoted to neutrino ph

sics, and the second part i

omposed of chapters 6—11 and devoted to neutrino astronomy and neutrino

osmolo

y.Weadmitthatitisabi

challen

or us to catch up with th

rapid developments in neutrino ph

sics, neutrino astronom

and neutrino

osmology, which are partly characterized by the rising number of publica-

tions everyday.

lthou

h we have tried to cover recent pro

ress in neutrino

cience, a lot of interesting materials and technical details have to be skippe

rom this book for a given page limitation. We apologize for missing many

usefu

efe

ces fo

esa

easo

e are deeply indebted to our families for their understanding and sup-

port durin

the writin

this book. We would like to thank many o

ollaborators and collea

ues who kindly allow us to quote some tables,

ﬁg-

res and physical results from their papers. One of us

(

Z.Z.X.

)

is gratefu

to Harald Fritzsch

or collaboratin

on his

ﬁ

rst scienti

ﬁ

c paper on neutrino

asses in September 1995. One of us

(

S.Z.

)

is grateful to Georg G. Raﬀel

or suggesting the present title of this book and for his encouragement and

ospita

at t

eMax-P

anc

-Institute in Munic

.Wewou

eto

thank the editorial staﬀ of Zhejian

University Press and Sprin

er Verla

for

nviting us to write t

coming to our assistance. T

is wor

was

upportedinpartb

the National Natural

cience Foundation o

hina un

er grant No. 10425522 and No. 10875131

(

Z.Z.X.

)

,inpartbytheMinistry

of Science and Technology of China under grant No. 2009CB825207

(

Z.Z.X.

)

nd in part by the Alexander von Humboldt Foundation of Germany

(

S.Z.

Zhi-Zhong Xin

eijin

ust 201

hun Zho

Munich,

ust 201

ontents

1 Neutrinos: Past

Present and Future

...................... 1

.1 Neutrinos in Nuc

ear an

Partic

ysics ................

1.1.1 Pau

’

sNeutrinoH

pot

esis ......................

1.1.2 Weak Interactions and Neutrinos ..................

1.1.

Discoveriesof Neutrinos..........................

.2 Neutrinos in

stronomy and Cosmolo

y..................

1.2.1 Neutrinos from Stars and Su

ernovae ..............

1.2.2 High-energyCosmic Neutrinos .....................

1.2.3

osmic Neutrino Back

round ......................

.3 Knowledge and QuestionsonNeutrinos ..................

1.3.1 Present Know

geonNeutrinos ...................

1.3.2

uestions onNeutrinos .....................

eferences ................................................

2 Neutrinos within the

tandard Mode

...................

.1 Fundamentals o

the

tandardModel ....................

2.1.1 GaugeSymmetries ..............................

2.1.2

pontaneous

ymmetry Breakin

..................

2.1.3 Renormalizabilit

...............................

2.1.4 The

tandardElectroweakModel .................

tandard Interactions o

Neutrinos.......................

2.2.1 Neutrino-electron Scatterin

......................

2.2.2 Neutrino-neutrinoScattering......................

2.2.

Neutrino-nuc

eonInteractions.....................

.3 Neutrino Propa

ationin aMedium .......................

2.3.1 Coherent ForwardScattering......................

2.3.2 The E

ﬀ

ective Potential...........................

2.3.3 Neutrino Self-energy

pproach....................

eferences ................................................